\begin{abstract}

          A mapping study towards \numsou Planck Cold Clumps was made with \coaa, \cobb and \cocc lines, at the 13.7 m telescope of Purple Mountain Observatory. For all the clumps, \coaa and \cobb emissions were detected, while for \numcocc of them, \cocc emissions were detected.  Of the \numsou Clumps, \numsoutmc are in Taurus Molecular Complex (TMC), \numsoucmc in California  Molecular Complex (CMC) and \numsoupmc are in Perseus Molecular Complex (PMC). In the \numvelcomp velocity components, \numcore cores are found in \numcompofcores clumps, \numcoretmc cores are in TMC, \numcorecmc in CMC and \numcorepmc are in PMC.
          We acquired the observational parameters such as $V_{lsr}$, $T_{A}$ and FWHM of lines. Physical parameters including \texc, \nhyd, \sigmath, \sigmant,  \sigmatd were calculated.
          We found that most of the cores have \sigmant larger than \sigmath. Most cores are found with $M_{vir}$ and $M_J$ larger than $M_{LTE}$, indicating these cores are neither going to collapse nor gravitationally bound.
          To compare with the dust properties revealed by Planck ECC catalog, we investigated the coupling of gas and dust components. We found most of the cores are with dust temperature higher than gas temperature. Also, the objects associated with our sources are checked, for most of the core, no associated objects are found within distance of 55\arcsec to their centers.


\end{abstract}
\keywords{ISM:molecular-ISM:kinematics-Low mass stars:formation}
